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Dust grains with sizes around (sub)mm are expected to couple only weakly tothe gas motion in regions beyond 10 au of circumstellar disks. In this work, weinvestigate the influence of the spatial distribution of such grains on the(sub)mm appearance of magnetized protoplanetary disks. We perform non-idealglobal 3D magneto-hydrodynamic stratified disk simulations including particlesof different sizes (50 micron to 1 cm), using a Lagrangian particle solver. Wecalculate the spatial dust temperature distribution, including the dynamicallycoupled submicron-sized dust grains, and derive ideal continuum re-emissionmaps of the disk through radiative transfer simulations. Finally, weinvestigate the feasibility to observe specific structures in the thermalre-emission maps with the Atacama Large Millimeter/submillimeter Array (ALMA).The pressure bump close to the outer edge of the dead-zone leads to particletrapping in ring structures. More specifically, vortices in the diskconcentrate the dust and create an inhomogeneous distribution of the solidmaterial in the azimuthal direction. The large-scale disk perturbations arepreserved in the (sub)mm re-emission maps. The observable structures are verysimilar to those expected to result from planet-disk interaction. The largerdust particles increase the brightness contrast between gap and ringstructures. We find that rings, gaps and the dust accumulation in the vortexcould be traced with ALMA down to a scale of a few astronomical units incircumstellar disks located in nearby star-forming regions. Finally, we presenta brief comparison of these structures with those recently found with ALMA inthe young circumstellar disks of HL Tau and Oph IRS 48.

Gaps, rings, and non-axisymmetric structures in protoplanetary disks - Emission from large grains